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Nonlinear Calculations for BL Her Stars

Published online by Cambridge University Press:  12 April 2016

S. W. Hodson ,
A. N. Cox  and
D. S. King
S. W. Hodson
Affiliation:
Theoretical Division, Los Alamos Scientific Laboratory University of California, Los Alamos, NM 87545
A. N. Cox
Affiliation:
Theoretical Division, Los Alamos Scientific Laboratory University of California, Los Alamos, NM 87545
D. S. King
Affiliation:
Department of Physics & Astronomy, University of New Mexico, Albuquerque, NM

Extract

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BL Her Stars are primarily Population II Cepheids with periods between one and three days. On the H-R diagram they are about 1mbrighter than the RR Lyrae variables but below the W Virginis variables. They are not as blue as the so-called anomalous Cepheids. Typically these stars are metal deficient, but notable exceptions are the prototype BL Her and V553 Cen with solar type abundances (Smith, et al. 1978). Their evolutionary status given by Sweigart and Gross (1976) puts them on the immediate post-horizontal-branch stage with energy supplied by both He and H burning shells.

Type
VII. RR Lyrae and BL Herculis Variables
Information
International Astronomical Union Colloquium , Volume 58: Stellar Hydrodynamics , August 1980 , pp. 503 - 508
Copyright
Copyright © Reidel 1980

References

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